HR 8799 b

Size comparison of HR 8799 b (gray) with Jupiter.
Discovery
Discovered by	Marois et al.
Discovery site	Keck and Gemini observatories in Hawaii
Discovery date	November 13, 2008
Detection method	Direct imaging
Orbital characteristics
Semi-major axis	~ 68 AU
Orbital period (sidereal)	~ 460[1][note 1][note 2] y
Star	HR 8799
Physical characteristics
Mean radius	1.2 ± 0.1[1] RJ
Mass	5+2 −1[2] MJ
Mean density	5.041 g/cm3[3]
Temperature	870+30 −70[1]

HR 8799 b is an extrasolar planet located approximately 129 light-years away in the constellation of Pegasus, orbiting the 6th magnitude Lambda Boötis star HR 8799. It has a mass between 4 and 7 ^[2]Jupiter masses and a radius from 10 to 30% larger than Jupiter's. It orbits at 68 AU from HR 8799 (or 7 AU inside the inner edge of the dust disk orbiting the star) with an unknown eccentricity and a period of 460 years, and is the outermost known planet in the HR 8799 system. Along with two other planets orbiting HR 8799, the planet was discovered on November 13, 2008 by Marois et al., using the Keck and Gemini observatories in Hawaii. These planets were discovered using the direct imaging technique.^{[1][4][5][6][7]}

In 2009 it was discovered that the Hubble Space Telescope had in fact directly imaged HR 8799 b eleven years earlier, in 1998, suggesting that more exoplanets might be revealed through analysis of HST photographic archives.^[8] Additional precovery images were also obtained by reanalyzing data taken in 2002 at the Subaru Telescope and in 2005 and 2007 at the W. M. Keck Observatory.^[9][10][11]

Broadband photometry of HR 8799 b shows that it has thicker clouds in its atmosphere than do older, higher surface gravity substellar objects of the same effective temperature.^[12]

Near infrared H band and K band spectroscopy of HR 8799 b published in May 2011 indicate a hydrogen rich, dusty atmosphere with disequilibrium CO / CH₄ chemistry.^[13]

Near infrared spectroscopy made with the Palomar Observatory show evidence of ammonia and/or acetylene as well as carbon dioxide, and some methane.^[14] In 2015, the signals of water, carbon monoxide and methane were reported in infrared spectra taken at the Keck telescope.^[15] However, a reanalysis of the same data in 2018 shows that water and carbon monoxide are present, but that the methane detection may have been spurious. Observations by the James Webb Space Telescope will be capable of confirming or disproving the presence of methane in HR 8799 b's atmosphere.^[16]

• Fomalhaut b

Media related to HR 8799 b at Wikimedia Commons

• "HR 8799 b". Exoplanets. Archived from the original on 2012-03-04. Retrieved 2008-12-02.